Scale and the differential structure of images

Florack, Luc; Romeny, Bart M. ter Haar; Koenderink, Jan J.; Viergever, Max A.

doi:10.1016/0262-8856(92)90024-w

Cited by 331 publications

(199 citation statements)

References 18 publications

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“…At z = 1, the GSMF has been analysed in detail, through a wide variety of spectroscopic surveys. For example, Fontana et al (2004) (Guzzo et al, 2014). All these works consistently find that the high-mass end of the GSMF is dominated by red, quiescent galaxies, in complete agreement to what found in the local Universe.…”

Section: The Galaxy Stellar Mass Function In Different Environmentsmentioning

confidence: 99%

The Role of the Environment on Galaxy Evolution

Boselli

2011

A Panchromatic View of Galaxies

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Esame finale anno 2016A Milena "Che fai tu, Luna, in ciel? Dimmi, che fai, silenziosa Luna?" -Giacomo Leopardi, Canto notturno di un pastore errante dell'Asia A B S T R A C TAlthough the general picture of how galaxies have formed and evolved through cosmic time is already in place, still many details are missing. An example is represented by a quantitative characterization of the role that environment plays during the evolution of galaxies in determining their observed properties in the local Universe. Local galaxy environment has been thoroughly explored through observations at low redshift and it has recently started to being investigated also in the distant Universe. Moreover, general attention has been increasingly focused on the relation between galaxy evolution and galaxy positions with respect to the large-scale structures of the cosmic web.This work explores how environment (defined both in terms of local overdensities on the Mpc scale around galaxies, as well as in terms of the distribution of galaxy distances from ∼ 10 2 Mpc long cosmic filaments) is observationally related to galaxy properties such as their stellar mass, their star-formation activity, or the presence of Active Galactic Nucleus phenomena. The analysis reported here is performed in a large redshift range, going from the local Universe (z 0.2) to intermediate (z ∼ 0.7) and high-redshifts (z 3). To perform this study, both spectroscopic redshift data sets as well as photometric redshift surveys have been deployed and (particularly for the photometric redshift data sets) a thorough analysis of the effect of their observational issues on the measurement of local and global environment has been executed.The picture that emerges is that high-density environments are favoured places for galaxy evolution, showing an enhanced fraction of massive galaxies which have stopped forming stars and belong to the quiescent population. Galaxies in high-density environments have an increased probability of hosting radio-AGNs (belonging to the ensemble of processes that turn off the star-formation in massive galaxies) and these effects are visible since the start of the decline in the cosmic star-formation history. Large-scale structures, such as the filaments of the cosmic web, have also a role in shaping galaxy evolution and they may represent key places for the pre-processing of galaxies before they enter higher density regions such as the cluster or group environment.As an increasing amount of observational evidence on the relation between the evolution of galaxies and their environment is gathered, a complete solution to the problem of how the local galaxy population has evolved approaches, and the history of galaxies from their formation at the dawn of time to the present day gets closer to being traced. Figure 2 Growth of structures . . . . . . . . . . . . . . . 7 Figure 3 Evolution of the global SFR density . . . . . . . 8 Figure 4 Colour-density relation for VVDS galaxies . . 11 Figure 5 Fraction of M * contained in galaxies as a function sSFR ....

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Section: The Galaxy Stellar Mass Function In Different Environmentsmentioning

confidence: 99%

The Role of the Environment on Galaxy Evolution

Boselli

2011

A Panchromatic View of Galaxies

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“…Many other examples of the use of differential image structure by both machine and biological vision researchers can be found in the literature (e.g. Koenderink, 1984;Koenderink andvan Doorn, 1990, Koenderink andvan Doorn, 1994;Deriche et al, 1992;Deriche and Giraudon, 1993;Florack et al, 1992;Malik, 1987, Perona andMalik, 1990;Beaudet, 1978, Kitchen andRosenfeld, 1982;Krueger and Phillips, 1989).…”

Section: Introductionmentioning

confidence: 99%

The Local Structure of Space-variant Images

1997

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“…A systematic approach that has been developed to restrict the class of possibilities is to assume that the rst stages of visual processing should be as uncommitted as possible and have no particular bias. The essence of the results from scale-space theory (Witkin 1983Koenderink and van Doorn 1990Florack et al 1992Lindeberg 1994a) is that within the class of linear operations, convolution with Gaussian kernels and their derivatives is singled out as a canonical choice.…”

Section: Measuring a Ne Transformationsmentioning

confidence: 99%

Direct estimation of affine image deformations using visual front-end operations with automatic scale selection

Lindeberg

Proceedings of IEEE International Conference on Computer Vision

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This article deals with the problem of estimating deformations of brightness patterns using visual front-end operations. Estimating such deformations constitutes an important subtask in several computer vision problems relating to image correspondence and shape estimation. The following subjects are t r eated:The problem of decomposing a ne ow elds into simpler components is analysed in detail. A canonical parametrization is presented b ased on singular value decomposition, which naturally separates the rotationally invariant components of the ow eld from the rotationally variant ones.A novel mechanism is presented for automatic selection of scale levels when estimating local a ne deformations. This mechanism is expressed within a multiscale framework where d i s p arity estimates are c omputed in a hierarchical coarse-to-ne manner and corrected using iterative techniques. Then, deformation estimates are selected f r om the scales that minimize a certain normalized r esidual over scales. Finally, the descriptors so obtained serve as initial data for computing re ned estimates of the local deformations.

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Scale and the differential structure of images

Cited by 331 publications

References 18 publications

The Role of the Environment on Galaxy Evolution

The Role of the Environment on Galaxy Evolution

The Local Structure of Space-variant Images

Direct estimation of affine image deformations using visual front-end operations with automatic scale selection

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